Abstract
Since its discovery in 1955, Jupiter decametric emission has been extensively studied with ground-based instruments1, and more recently by planetary radioastronomy experiment on board the Voyager spacecraft2,3. However, we are still far from understanding the origin of the emission, mainly because we have no direct information about the position and structure of the source, due to the low spatial resolution of instruments at those wavelengths. Previous theories have assumed that the source emission takes place along magnetic field lines, close to the local gyrofrequency. We propose here a method to test this hypothesis by studying interplanetary scintillations which modulate the emission when received on Earth, and quantify the predicted effects. Preliminary results indicate that the emission is probably spatially distributed and could occur along field lines, and that Io controlled A and B sources are on opposite sides of Jupiter.
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Genova, F., Boischot, A. Structure of the source of jovian decametric emission and interplanetary scintillation. Nature 293, 382–383 (1981). https://doi.org/10.1038/293382a0
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DOI: https://doi.org/10.1038/293382a0
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